The knowledge of the dark matter (DM) velocity distribution is an important element of several types of DM searches e.g. direct detection, p-wave-suppressed or Sommerfeld-enhanced annihilating DM. Many predictions for these signals rely on a Maxwell-Boltzmann approximation for the velocity distribution, however a more refine calculation can be obtained using the Eddington inversion method. I will review the theoretical foundations of this technique as well as some of its shortcomings, then present a recent test of its reliability against hydrodynamical cosmological simulations.
MPP Astroparticle Physics Seminar